Measuring the sizes of stars

The Chatterton Astronomy Department aims to apply interferometers with very high resolving power to optical astronomy. The programme of the stellar intensity interferometer at Narrabri Observatory was completed in 1972 and since then the work has been directed towards building a more sensitive instrument with higher resolving power. As a first step a much larger intensity interferometer was designed but was not built because it was large, expensive and not as sensitive as desired. Efforts are now being made to design a more sensitive and cheaper instrument. A version of Michelson’s stellar interferometer is being built using modern techniques. It is hoped that it will reach stars of magnitude +8 and will work reliably in the presence of atmospheric scintillation. It is expected to cost considerably less than an intensity interferometer of comparable performance. The pilot model of this new instrument is almost complete and should be ready for test in 1984. Text of an Academy Lecture delivered at the Raman Research Institute, Bangalore on January 27, 1984.     

Numerical simulations of a Mars geodesy network experiment: Effect of orbiter angular momentum desaturation on Mars' rotation estimation

The scientific objectives of a geodetic experiment based on a network of landers, such as NEIGE (NEtlander Ionosphere and Geodesy Experiment) are to improve the current knowledge of Mars' interior and atmosphere dynamics. Such a network science experiment allows monitoring the motions of the Martian rotation axis with a precision of a few centimeters (or milli-arc-seconds (mas)) over annual and sub-annual periods. Thereto, besides radio tracking of a Mars orbiter from the Earth, radio Doppler shifts between this orbiter and several landers at the planet's surface will be performed. From the analysis of these radio Doppler data, it is possible to reconstruct the orbiter motion and Mars' orientation in space. The errors on the orbit determination (position and velocity of the orbiter) have an impact on the geodetic parameters determination from the Doppler shifts and must be removed from the signal in order to achieve a high enough accuracy. In this paper, we perform numerical simulations of the two Doppler signals involved in such an experiment to estimate the impact of the spacecraft angular momentum desaturations on the determination of Mars' orientation variations. The attitude control of the orbiter needs such desaturation maneuvers regularly repeated. They produce velocity variations that must be taken into account when determining the orbit. For our simulations, we use a priori models of the Martian rotation and introduce the spacecraft velocity variations induced by each desaturation event. By a least-squares adjustment of the simulated Doppler signals, we then estimate the orbiter velocity variations and the parameters of the Mars' rotation model. We show that these velocity variations are ill resolved when the spacecraft is not tracked, therefore requiring a near-continuous tracking from the Earth to accurately determine the orbit. In such conditions we show that only 15- of lander-orbiter tracking per week allows recovering Mars' orientation parameters with a precision of a few mas over a period of 1 Martian year.     

北京北郊冬季大风过程湍流通量演变特征的分析研究

利用中国科学院大气物理研究所325 m气象观测塔1993年12月～1994年1月大气边界层实验资料, 计算分析了大风过境过程中47 m和120 m高度湍流通量演变特征及其影响因子, 以及与风速、 稳定度等参数的关系。结果表明: 大风过程对近地面层的物质能量输送有着重要影响, 大风之前出现短时间动量上传和热量下传; 大风过程中的湍流通量数值明显高于过境后, 水平方向湍流通量数值和能量增加幅度大于垂直方向; 当风速大于临界值5 m/s时, 湍流通量与风速、 湍流动能的相关迅速增大; 湍流谱特征表现为湍流能量的低频部分增加、 湍流谱曲线变宽; 大风能强烈影响近地面层的能量收支。     

Detection of non-radial pulsation and faint companion in the symbiotic star CH Cyg

We have detected asymmetry in the symbiotic star CH Cyg through the measurement of precision closure phase with the Integrated Optics Near-Infrared Camera (IONIC) beam combiner, at the infrared optical telescope array interferometer. The position of the asymmetry changes with time and is correlated with the phase of the 2.1-year period found in the radial velocity measurements for this star. We can model the time-dependent asymmetry either as the orbit of a low-mass companion around the M giant or as an asymmetric, 20 per cent change in brightness across the M giant. We do not detect a change in the size of the star during a 3-year monitoring period neither with respect to time nor with respect to wavelength. We find a spherical dust shell with an emission size of 2.2 ± 0.1 D _* full width at half-maximum around the M giant star. The star to dust flux ratio is estimated to be 11.63 ± 0.3. While the most likely explanation for the 20 per cent change in brightness is non-radial pulsation, we argue that a low-mass companion in close orbit could be the physical cause of the pulsation. The combined effect of pulsation and low-mass companion could explain the behaviour revealed by the radial velocity curves and the time-dependent asymmetry detected in the closure-phase data. If CH Cyg is a typical long secondary period variable then these variations could be explained by the effect of an orbiting low-mass companion on the primary star.     

Optimizing point-source parameters for scanning satellite surveys

We describe a method for deriving the position and flux of point and compact sources observed by a scanning survey mission. Results from data simulated to test our method are presented, which demonstrate that at least a 10-fold improvement is achievable over that of extracting the image parameters, position and flux, from the equivalent data in the form of pixel maps. Our method achieves this improvement by analysing the original scan data and performing a combined, iterative solution for the image parameters. This approach allows for a full and detailed account of the point-spread function (PSF), or beam profile, of the instrument. Additionally, the positional information from different frequency channels may be combined to provide the flux-detection accuracy at each frequency for the same sky position. Ultimately, a final check and correction of the geometric calibration of the instrument may also be included. The Planck mission was used as the basis for our simulations, but our method will be beneficial for most scanning satellite missions, especially those with non-circularly symmetric PSFs.     

Unveiling the chemistry of hot protostellar cores with ALMA

High angular resolution mm-wave observations of the Orion-KL region, made with the IRAM Plateau de Bure interferometer (PdBI), reveal the presence of several cores of size 10³ AU, which have distinct spectral signatures. Complex molecules such as ethanol, vinyl cyanide and dimethyl ether show different distributions and their relative abundance varies from core to core by orders of magnitude. The molecular column densities derived in the cores also differ widely from the beam-averaged column densities observed with large single-dish telescopes. Obviously, the predictions of hot core chemistry models must be checked against high resolution observations. ALMA, which allies sensitivity and high angular resolution, will be a key instrument for this type of studies. The PdBI observations were part of a search for interstellar glycine, also carried out with the IRAM 30-m telescope and the Green Bank Telescope. We derive a 3σ upper limit on the column density of glycine of 1×10¹⁵ cm⁻² per 2″×3″ beam in the Orion Hot Core and Compact Ridge. Based on observations made with the IRAM PdB Interferometer, the IRAM 30-m telescope and the NRAO Green-Bank telescope. IRAM is supported by CNRS, MPG and IGN.     

LOLAS: an optical turbulence profiler in the atmospheric boundary layer with extreme altitude resolution

We report the development and first results of an instrument called Low Layer SCIDAR (Scintillation Detection and Ranging) (LOLAS) which is aimed at the measurement of optical-turbulence profiles in the atmospheric boundary layer with high altitude resolution. The method is based on the Generalized SCIDAR (GS) concept, but unlike the GS instruments which need a 1-m or larger telescope, LOLAS is implemented on a dedicated 40-cm telescope, making it an independent instrument. The system is designed for widely separated double-star targets, which enables the high altitude resolution. Using a 200-arcsec-separation double star, we have obtained turbulence profiles with unprecedented 12-m resolution. The system incorporates necessary novel algorithms for autoguiding, autofocus and image stabilization. The results presented here were obtained at Mauna Kea Observatory. They show LOLAS capabilities but cannot be considered as representative of the site. A forthcoming paper will be devoted to the site characterization. The instrument was built as part of the Ground Layer Turbulence Monitoring Campaign on Mauna Kea for Gemini Observatory.     

顾及大气角动量的Prophet-VAR日长变化预报方法

针对日长变化参数序列中蕴含的复杂非线性特征会严重影响其预报精度的问题,同时为探讨引入大气角动量序列是否有助于提升预报精度,提出一种Prophet拟合外推联合向量自回归(vector autoregression,VAR)残差补偿的组合模型用于日长预报.选用2008～2020年的日长变化参数序列进行实验,同时设计不顾及大...     

资源三号卫星多光谱影像的姿态角常差检校

针对资源三号卫星姿态角常差导致的多光谱影像定位精度降低的问题,该文在构建多光谱影像严格几何定位模型的基础上,提出了运用罗德里格矩阵建立姿态角常差检校方法;根据少量地面控制点求出姿态角常差构成的偏置矩阵后,使影像定位精度得到显著提高。实验结果证明,该方法具有较好的应用价值。     

雷暴大风过程中对流层中低层动量通量和动能通量输送特征研究

2014年5月31日北京发生一次雷暴大风过程。以雷达资料同化结果为初始场,对此次过程进行高分辨率数值模拟。采用非静力平衡和非地转平衡的经向动量方程和质量权重动能方程,利用模拟资料,对雷暴大风过程中经向动量和质量权重动能进行收支分析,以此来研究雷暴过程中对流层中低层动量通量和动能通量输送特征,讨论地面大风的可能成因。分析结果表明,在对流层中低层,经向动量通量散度是影响经向动量局地变化的主要强迫项。雷暴系统后部的入流把中低层的经向动量倾斜向下输送,系统前部对流云区中低层的下沉气流也向下输送经向动量。这两支下传动量通量先后与近地面经向动量的水平通量汇合,向系统前沿输送经向动量。在北京西北部地形阻挡作用下,经向动量通量在系统前端近地面辐合,促进那里的经向动量局地增长,有利于增强那里的南风。质量动能收支的特征与经向动量收支类似,在近地面层质量动能的局地变化主要是由质量动能通量散度引起的。系统后部入流把中层质量动能向下传输到近地面层,然后与近地面质量动能的水平通量汇合,向系统前沿输送质量动能。相对来说,近地面层经向动量和质量动能的水平通量比下传通量更重要,这主要与低层较强的东南急流有关。